In this paper we use the term coronal bright front [1]} to refer to the phenomenon that can be described as a shock wave, shock front, or bright front, defined as the anti-sunward edge of the shock sheath.
According to numerous previous studies [2]}, [1]}, the best SDO/AIA channels for observing CBFs are the ones centered on 193Å and 211Å wavelengths. In this work, we use 193Å data. The data is initially obtained via a standard AIA pipeline using SunPy package [4]}.
